Interstellar lines in spectra of extragalactic sources. III Markarian 509, Arakelian 120, and 3C 273

York, D. G.; Ratcliff, S. J.; Blades, J. C.; Cowie, L. L.; Morton, Donald C.; Wu, Chin‐Chun

doi:10.1086/161595

Cited by 15 publications

(10 citation statements)

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“…Our FOS observations found the same two kinematic components as those identiÐed by York et al (1984) D12 yr earlier, and we found N V at these velocities as well (Crenshaw et al 1995). We originally agreed with the suggestion of York et al (1984) that these components arise from extended regions of ionized gas in the host galaxy.…”

Section: A6 Ngc 5548supporting

confidence: 89%

“…We originally agreed with the suggestion of York et al (1984) that these components arise from extended regions of ionized gas in the host galaxy. However the high-resolution GHRS spectra of Lya (also shown in Savage et al 1997) demonstrates that these two components are broad and are likely to arise close to the nucleus.…”

Section: A6 Ngc 5548supporting

confidence: 87%

“…Mrk 509 York et al (1984) found two kinematic components of intrinsic Lya and C IV absorption in high-dispersion IUE spectra. Evidence for an X-ray warm absorber is given by Reynolds (1997) and George et al (1998b).…”

Section: A6 Ngc 5548mentioning

confidence: 99%

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Intrinsic Absorption Lines in Seyfert 1 Galaxies. I. Ultraviolet Spectra from theHubble Space Telescope

Crenshaw

Kraemer

Boggess³

et al. 1999

ApJ

311

366

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We present a study of the intrinsic absorption lines in the ultraviolet spectra of Seyfert 1 galaxies. The study is based on spectra from the Hubble Space T elescope and includes the Seyfert 1 galaxies observed with the Faint Object Spectrograph and Goddard High-Resolution Spectrograph at spectral resolutions of j/*j B 1000È20,000 with good signal-to-noise ratios. We Ðnd that the fraction of Seyfert 1 galaxies that show intrinsic absorption associated with their active nuclei is more than one-half (10 of 17), which is much higher than previous estimates (3%È10%) based on IUE data. There is a one-to-one correspondence between Seyfert galaxies that show intrinsic UV absorption and X-ray "" warm absorbers, ÏÏ indicating that these two phenomena are related. Although our sample is not complete, we conclude that intrinsic absorption represents an important component that needs to be integrated into our overall physical picture of active galaxies. The intrinsic UV absorption is generally characterized by high ionization : C IV and N V are seen in all 10 Seyfert galaxies with detected absorption (in addition to Lya), whereas Si IV is present in only four of these Seyfert galaxies, and Mg II absorption is detected only in NGC 4151. The absorption lines are blueshifted (or in a few cases at rest) with respect to the narrow emission lines, indicating that the absorbing gas is undergoing net radial outÑow. At high resolution, the absorption often splits into distinct kinematic components that show a wide range in widths (20È400 km s~1 FWHM), indicating macroscopic motions (e.g., radial velocity subcomponents or turbulence) within a component. The strong absorption components have cores that are much deeper than the continuum Ñux levels, indicating that the regions responsible for these components lie completely outside of the broad emission-line regions. Additional information on the covering factors and column densities can be derived from the absorption proÐles in the high-resolution spectra. The covering factor of the absorbing gas in the line of sight, relative to the total underlying emission, is on average. The global C los º 0.86, covering factor, which is the fraction of emission intercepted by the absorber averaged over all lines of sight, is Thus, structures covering large solid angles as seen by the central continuum source C global º 0.5. (e.g., spherical shells, sheets, or cones with large opening angles) are required. The individual absorption components show a wide range in C IV column densities (0.1È14 ] 1014 cm~2), and the ratio of N V to C IV column density varies signiÐcantly from one absorption component to the next, even in the same Seyfert galaxy. Thus, the intrinsic absorption in a Seyfert 1 galaxy is typically comprised of distinct kinematic components that are characterized by a range in physical conditions (e.g., ionization parameter and hydrogen column density). Finally, we show evidence for extreme variability in the intrinsic absorption lines of NGC 3783. In addition to our earlier repo...

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Section: A6 Ngc 5548supporting

confidence: 89%

Section: A6 Ngc 5548supporting

confidence: 87%

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Intrinsic Absorption Lines in Seyfert 1 Galaxies. I. Ultraviolet Spectra from theHubble Space Telescope

Crenshaw

Kraemer

Boggess³

et al. 1999

ApJ

311

366

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“…Mrk 509 is an ideal object for study due to its high flux, moderate luminosity that rivals that of QSOs (Kopylov et al 1974), and deep, well structured absorption troughs. The blue-shifted absorption indicative of a nuclear outflow has been known since the earliest UV spectral observations (Wu et al 1980;York et al 1984). The outflow is also apparent in the blueshifted [O iii] emission detected across the face of Mrk 509 by Phillips et al (1983).…”

Section: Introductionmentioning

confidence: 87%

Multiwavelength campaign on Mrk 509

Kriss

Arav

Kaastra

et al. 2011

A&A

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We present medium-resolution (λ/Δλ ∼ 20 000) ultraviolet spectra covering the 1155−1760 Å spectral range of the Seyfert 1 galaxy Mrk 509 obtained using the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope (HST). Our observations were obtained simultaneously with a Low Energy Transmission Grating Spectrometer observation using the Chandra X-ray Observatory, and they are part of a multiwavelength campaign in September through December 2009 which also included observations with XMM-Newton, Swift, and INTEGRAL. Our spectra are the highest signal-to-noise observations to date of the intrinsic absorption components seen in numerous prior ultraviolet observations. To take advantage of the high S/N, we describe special calibrations for wavelength, flat-field and line-spread function corrections that we applied to the COS data. We detect additional complexity in the absorption troughs compared to prior observations made with the Space Telescope Imaging Spectrograph (STIS) on HST. We attribute the UV absorption to a variety of sources in Mrk 509, including an outflow from the active nucleus, the interstellar medium and halo of the host galaxy, and possible infalling clouds or stripped gaseous material from a merger that are illuminated by the ionizing radiation of the active nucleus. Variability between the STIS and COS observation of the most blue-shifted component (#1) allows us to set an upper limit on its distance of <250 pc. Similarly, variability of component 6 between FUSE observations limits its distance to <1.5 kpc. The absorption lines in all components only partially cover the emission from the active nucleus with covering fractions that are lower than those seen in the prior STIS observations and are comparable to those seen in spectra from the Far Ultraviolet Spectroscopic Explorer (FUSE). Given the larger apertures of COS and FUSE compared to STIS, we favor scattered light from an extended region near the active nucleus as the explanation for the partial covering. As observed in prior X-ray and UV spectra, the UV absorption has velocities comparable to the X-ray absorption, but the bulk of the ultraviolet absorption is in a lower ionization state with lower total column density than the gas responsible for the X-ray absorption. We conclude that the outflow from the active nucleus is a multiphase wind.

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“…Ground-based reverberation mapping using optical spectra (Peterson et al 1998(Peterson et al , 2004Kaspi et al 2000) established a black-hole mass of 1.1 × 10 8 M (Bentz & Katz 2015). The earliest IUE observations (Wu et al 1980;York et al 1984) revealed the blueshifted UV absorp-All COS and FUSE spectra used in the paper are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/ 623/A82 tion characteristic of AGN outflows. These features were studied at more detail and at higher spectral resolution with the Far Ultraviolet Spectroscopic Explorer (FUSE; Kriss et al 2000) and the Space Telescope Imaging Spectrograph (STIS) on the Hubble Space Telescope (HST; Kraemer et al 2003).…”

Section: Introductionmentioning

confidence: 99%

Multiwavelength campaign on Mrk 509

Kriss

Arav

Edmonds

et al. 2019

A&A

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Aims. To elucidate the location, physical conditions, mass outflow rate, and kinetic luminosity of the outflow from the active nucleus of the Seyfert 1 galaxy Mrk 509, we used coordinated UV and X-ray spectral observations in 2012 to follow up our lengthier campaign conducted in 2009. Methods. We observed Mrk 509 with the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope (HST) on 2012-09-03 and 2012-10-11 coordinated with X-ray observations using the High Energy Transmission Grating on the Chandra X-ray Observatory. Our far-ultraviolet spectra used grating G140L on COS to cover wavelengths from 920–2000 Å at a resolving power of ∼2000, and gratings G130M and G160M to cover 1160–1750 Å at a resolving power of ∼15, 000. Results. We detect variability in the blueshifted UV absorption lines on timescales spanning 3–12 years. The inferred densities in the absorbing gas are greater than log n cm−3 ∼ 3. For ionization parameters ranging over log U = −1.5 to −0.2, we constrain the distances of the absorbers to be closer than 220 pc to the active nucleus. Conclusions. The impact on the host galaxy appears to be confined to the nuclear region.

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Interstellar lines in spectra of extragalactic sources. III Markarian 509, Arakelian 120, and 3C 273

Cited by 15 publications

References 0 publications

Intrinsic Absorption Lines in Seyfert 1 Galaxies. I. Ultraviolet Spectra from theHubble Space Telescope

Intrinsic Absorption Lines in Seyfert 1 Galaxies. I. Ultraviolet Spectra from theHubble Space Telescope

Multiwavelength campaign on Mrk 509

Multiwavelength campaign on Mrk 509

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